Advances in Astronomy and Space Physics, Volume 5, Issue 2, PP. 93-98 (2015)
doi: 10.17721/2227-1481.5.93-98
doi: 10.17721/2227-1481.5.93-98
Magnetosheath and solar wind turbulence processes
features identification
features identification
1Taras Shevchenko National University of Kyiv, Glushkova ave. 4, 03127, Kyiv, Ukraine
2Johns Hopkins University Applied Physics Laboratory, Laurel MD, USA
2Johns Hopkins University Applied Physics Laboratory, Laurel MD, USA
Abstract
A different kind of analysis should be applied to a turbulent process, than that applied to a nondisturbed medium. In this work we present the result of extended self-similarity analysis (ESS) by comparing between different turbulent models: Kolmogorov K41 model, She-Leveque (isotropic log-Poisson model) of order 3; Iroshnikov-Kraichnan model and Politano-Pouquet model of order 4. Two regimes were observed for large and small timescales: the Gaussian distribution was used for small timescales for magnetic field fluctuation probability distribution function (PDF), and the Lévy distribution was used for large-scale timescale non-Gaussian distributions. The intersection of two asymptotes corresponds to approximately 1 s, which agrees with the ion-cyclotron period.
Keywords:
magnetopause, cusp, and boundary layers; solar wind-magnetosphere interactions; nonlinear phenomena